Résumé

Star formation in self-gravitating turbulent fluids

Norman Murray (CITA)

I will describe a model of star formation in self-gravitating
turbulent gas. I treat the turbulent velocity as a dynamical variable,
and assume that it is adiabatically heated by the collapse. The theory
predicts the run of density, infall velocity, and turbulent velocity,
and the rate of star formation. The turbulent pressure is dynamically
important at all radii, a result of the adiabatic heating powered by
the collapse. The density is given by a broken power law with a slope
-1.5 at small radii and ~1.7 at large radii. Both the turbulent velocity and the infall velocity decrease with decreasing radius at
large r. The accreted (stellar) mass grows as the square of the time.
I will show numerical simulations that verify the predictions
of the theory for the star formation rate, density, radial infall
velocity, and turbulent velocity.